We present results from a detailed analysis of a third eclipsing binary ( EB ) system in the Large Magellanic Cloud , EROS 1044 ( \sim B2 IV–V + \sim B2 III–IV ) .
Our study combines the ‘ ‘ classical ’ ’ EB study of light and radial velocity curves with detailed modeling of the observed spectral energy distribution , and yields an essentially complete picture of the stellar properties of the system and a determination of its distance .
The observational data exploited include optical photometry , space-based UV spectroscopy , and UV/optical spectrophotometry .
The advantages of our technique include numerous consistency checks and , in the case of the distance determinations , the absence of zero point uncertainties and adjustable parameters .
We find the EROS 1044 system to consist of a pair of normal , mildly-evolved \sim 21000 K stars , whose derived properties are consistent with stellar evolution calculations .
The distance to the system is 47.5 \pm 1.8 kpc .
We discuss the implications of our results for three EB systems ( HV 2274 , HV 982 , and EROS 1044 ) on the general distance to the Large Magellanic Cloud .